ALPINE is a \(69\,{\rm hour}\)  ALMA large program (\(\#\)  2017.1.00428.L) carried out in Cycles 5 and 6 in Band 7 (0.8–1.1 mm or 275–373 GHz). The program is a collaboration between several members of ALMA regional centers, including Europe, North America, Chile, and Japan. Of the 118 galaxies with spectroscopic redshifts of 4.4–5.9, 105 are located in the COSMOS field [1]} and 13 in the ECDFS [2]}. The sample spans roughly two orders of magnitude in stellar mass and SFR on the star-forming main-sequence, hence including a representative sample of typical main-sequence galaxies at these cosmic times (Figure REF ). The galaxies were selected in two redshift windows at \(4.40 < z < 4.65\)  (67 galaxies) and \(5.05 < z < 5.90\)  (51 galaxies) with median redshifts of \(z\)\(\sim \)\(4.5\)  and \(z\)\(\sim \)\(5.5\) , respectively. The windows were chosen to avoid frequencies of low atmospheric transmission and to optimize the observation efficiency. The spectroscopic redshifts were gathered from two large spectroscopic surveys carried out by Keck/DEIMOS (DEIMOS 10k Survey; [3]}) and VLT/VIMOS (VIMOS Ultra Deep Survey, VUDS; [4]}). These surveys combine redshifts of galaxies selected in a variety of ways, for example, by narrowband Ly\(\alpha \)  emission, Spitzer \(4.5\,{\rm {m}}\)  flux excess, Lyman Break color selection (LBGs), and photometric redshifts. This variety is inherited in the final ALPINE sample, emphasizing the selection of representative galaxies at these redshifts. Furthermore, the redshifts were derived from Ly\(\alpha \)  emission as well as UV absorption lines, therefore minimizing selection biases towards young, dusty-poor Ly\(\alpha \)  emitters. All spectra have been consistently renormalized using the COSMOS2015 photometric catalog [5]} or CANDELS photometry, using broadband and narrowband data (see [6]} for a full description). The ALPINE galaxies have an absolute rest-UV magnitude of \(M_{\rm 1500} > -20.2\,{\rm mag}\) , corresponding to an equivalent SFR of \(10\,{\rm {M}_{\odot }\,yr^{-1}}\) . This cut was chosen to maximize the number of C\(^+\)  line detections according to the \(L_{{\rm C^{+}}}\)  vs. \(M_{\rm 1500}\)  relation found in [7]} based on 10 \(z\)\(\sim \)\(5.5\)  galaxies with similar observations.
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